Detection of Flux Emergence, Splitting, Merging, and Cancellation of Network Field. I. Splitting and Merging

Iida, Yusuke; Hagenaar, H. J.; Yokoyama, T.

doi:10.1088/0004-637x/752/2/149

Cited by 38 publications

(43 citation statements)

References 25 publications

(45 reference statements)

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“…The fluxes follow a power law distribution of the form a x b with index b = −1.85 which is consistent with Parnell et al (2009). Other recent studies using Hinode data also obtain a power law index close to −1.8 (see e.g., Iida et al 2012;Buehler et al 2013, the focus of the former being the network fields).…”

Section: Distribution Of the Area Magnetic Field And Magnetic Flux Osupporting

confidence: 81%

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Statistical evolution of quiet-Sun small-scale magnetic features using Sunrise observations

Anusha¹,

Solanki²,

Hirzberger³

et al. 2017

A&A

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The evolution of small magnetic features in quiet regions of the Sun provides a unique window to probing solar magnetoconvection. Here we analyze small scale magnetic features in the quiet Sun, using the high resolution, seeing-free observations from the Sunrise balloon borne solar observatory. Our aim is to understand the contribution of different physical processes, such as splitting, merging, emergence and cancellation of magnetic fields to the rearrangement, addition and removal of magnetic flux in the photosphere. We employ a statistical approach for the analysis and the evolution studies are carried out using a feature tracking technique. In this paper we provide a detailed description of the feature tracking algorithm that we have newly developed and we present the results of a statistical study of several physical quantities. The results on the fractions of the flux in the emergence, appearance, splitting, merging, disappearance and cancellation qualitatively agrees with other recent studies (see e.g., Lamb et al. 2008Lamb et al. , 2013. To summarize, the total flux gained in unipolar appearance is an order of magnitude larger than the total flux gained in emergence. On the other hand, the bi-polar cancellation contributes nearly an equal amount to the loss of magnetic flux as unipolar disappearance. The total flux lost in cancellation is nearly 6 − 8 times larger than the total flux gained in emergence. One big difference between our study and previous similar studies is that thanks to the higher spatial resolution of Sunrise we can track features with fluxes as low as 9 × 10 14 Mx. This flux is nearly an order of magnitude lower than the smallest fluxes of the features tracked in the highest resolution previous studies based on Hinode data. The area and flux of the magnetic features follow power-law type distribution, while the lifetimes show either power-law or exponential type distribution depending on the exact definitions used to define various birth and death events. We also statistically determine the evolution of the flux within the features in the course of their lifetime, finding that this evolution depends very strongly on the birth and death process that the features undergo.

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Section: Distribution Of the Area Magnetic Field And Magnetic Flux Osupporting

confidence: 81%

“…9. Power-law fits to the histograms of the fluxes depend sensitively on the smallest flux per feature in the distribution (see also Parnell et al 2009;Iida et al 2012). …”

Section: Distribution Of the Area Magnetic Field And Magnetic Flux Omentioning

confidence: 99%

Statistical evolution of quiet-Sun small-scale magnetic features using Sunrise observations

Anusha¹,

Solanki²,

Hirzberger³

et al. 2017

A&A

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“…• How do the individual and statistical properties (e.g., Hagenaar, 2001;Hagenaar et al, 2003;Iida et al, 2012;Otsuji et al, 2011) of emerging flux relate to the solar activity cycle?…”

Section: Science Questions and Challenges In Flux Emergencementioning

confidence: 99%

Flux Emergence (Theory)

Cheung

Isobe

2014

Living Rev. Solar Phys.

190

175

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Magnetic flux emergence from the solar convection zone into the overlying atmosphere is the driver of a diverse range of phenomena associated with solar activity. In this article, we introduce theoretical concepts central to the study of flux emergence and discuss how the inclusion of different physical effects (e.g., magnetic buoyancy, magnetoconvection, reconnection, magnetic twist, interaction with ambient field) in models impact the evolution of the emerging field and plasma.

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“…Such features are continually evolving due to interactions with one another (Schrijver et al 1997;Parnell 2001; Thornton & Parnell 2011;Iida et al 2012) and the influence of underlying photospheric flows (Leighton et al 1962;Rieutord et al 2008;Rieutord & Rincon 2010).…”

Section: Introductionmentioning

confidence: 99%

THE STORAGE AND DISSIPATION OF MAGNETIC ENERGY IN THE QUIET SUN CORONA DETERMINED FROM SDO /HMI MAGNETOGRAMS

Meyer

Sabol

Mackay

et al. 2013

ApJ

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In recent years, higher cadence, higher resolution observations have revealed the quiet-Sun photosphere to be complex and rapidly evolving. Since magnetic fields anchored in the photosphere extend up into the solar corona, it is expected that the small-scale coronal magnetic field exhibits similar complexity. For the first time, the quiet-Sun coronal magnetic field is continuously evolved through a series of non-potential, quasi-static equilibria, deduced from magnetograms observed by the Helioseismic and Magnetic Imager on board the Solar Dynamics Observatory, where the photospheric boundary condition which drives the coronal evolution exactly reproduces the observed magnetograms. The build-up, storage, and dissipation of magnetic energy within the simulations is studied. We find that the free magnetic energy built up and stored within the field is sufficient to explain small-scale, impulsive events such as nanoflares. On comparing with coronal images of the same region, the energy storage and dissipation visually reproduces many of the observed features. The results indicate that the complex small-scale magnetic evolution of a large number of magnetic features is a key element in explaining the nature of the solar corona.

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Detection of Flux Emergence, Splitting, Merging, and Cancellation of Network Field. I. Splitting and Merging

Cited by 38 publications

References 25 publications

Statistical evolution of quiet-Sun small-scale magnetic features using Sunrise observations

Statistical evolution of quiet-Sun small-scale magnetic features using Sunrise observations

Flux Emergence (Theory)

THE STORAGE AND DISSIPATION OF MAGNETIC ENERGY IN THE QUIET SUN CORONA DETERMINED FROM SDO /HMI MAGNETOGRAMS

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